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An extensive spectroscopic time series of three Wolf-Rayet stars - I. The lifetime of large-scale structures in the wind of WR 134

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    0469454 - ASÚ 2017 RIV GB eng J - Journal Article
    Aldoretta, E.J. - St-Louis, N. - Richardson, N. - Moffat, A.F.J. - Eversberg, T. - Hill, G.M. - Shenar, T. - Artigau, E. - Gauza, B. - Knapen, J.H. - Kubát, Jiří - Kubátová, Brankica - Maltais-Tariant, R. - Munoz, M. - Pablo, H. - Ramiaramanantsoa, T. - Richard-Laferriere, A. - Sablowski, D.P. - Simon-Diaz, S. - St-Jean, L. - Bolduan, F. - Dias, F.M. - Dubreuil, P. - Fuchs, D. - Garrel, T. - Grutzeck, G. - Hunger, T. - Kuesters, D. - Langenbrink, M. - Leadbeater, R. - Li, D. - Lopez, A. - Mauclaire, B. - Moldenhawer, T. - Potter, M. - dos Santos, E.M. - Schanne, L. - Schmidt, J. - Sieske, H. - Strachan, J. - Stinner, E. - Stinner, P. - Stober, B. - Strandbaek, K. - Syder, T. - Verilhac, D. - Waldschlaeger, U. - Weiss, D. - Wendt, A.
    An extensive spectroscopic time series of three Wolf-Rayet stars - I. The lifetime of large-scale structures in the wind of WR 134.
    Monthly Notices of the Royal Astronomical Society. Roč. 460, č. 3 (2016), s. 3407-3417. ISSN 0035-8711. E-ISSN 1365-2966
    R&D Projects: GA ČR GA13-10589S
    Institutional support: RVO:67985815
    Keywords : instabilities * data analysis * spectroscopic techniques
    Subject RIV: BN - Astronomy, Celestial Mechanics, Astrophysics
    Impact factor: 4.961, year: 2016

    During the summer of 2013, a 4-month spectroscopic campaign took place to observe the variabilities in three Wolf-Rayet stars. The spectroscopic data have been analysed for WR 134 (WN6b), to better understand its behaviour and long-term periodicity, which we interpret as arising from corotating interaction regions (CIRs) in the wind. By analysing the variability of the He ii lambda 5411 emission line, the previously identified period was refined to P = 2.255 +/- 0.008 (s.d.) d. The coherency time of the variability, which we associate with the lifetime of the CIRs in the wind, was deduced to be 40 +/- 6 d, or similar to 18 cycles, by cross-correlating the variability patterns as a function of time. When comparing the phased observational grey-scale difference images with theoretical grey-scales previously calculated from models including CIRs in an optically thin stellar wind, we find that two CIRs were likely present.
    Permanent Link: http://hdl.handle.net/11104/0267257

     
     
Number of the records: 1  

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